期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 509, 期 3, 页码 3488-3503出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab3239
关键词
black hole physics; gravitational waves
资金
- European Union [818691]
- INFN [H45J18000450006]
- MIUR [PRIN 2017-MB8AEZ]
- [PGC2018-097585-B-C22]
The amplitude of the nano-Hz stochastic gravitational wave background resulting from an unresolved population of inspiralling massive black hole binaries is estimated. The model predicts an amplitude in agreement with current estimations and the contribution mainly comes from equal-mass binaries.
We estimate the amplitude of the nano-Hz stochastic gravitational wave background (GWB) resulting from an unresolved population of inspiralling massive black hole binaries (MBHBs). To this aim, we use the L-Galaxies semi-analytical model applied on top of the Millennium merger trees. The dynamical evolution of MBHBs includes dynamical friction, stellar and gas binary hardening, and gravitational wave (GW) feedback. At the frequencies proved by the Pulsar Timing Array experiments, our model predicts an amplitude of similar to 1.2 x 10(-15) at similar to 3 x 10(-8) Hz in agreement with current estimations. The contribution to the background comes primarily from equal-mass binaries with chirp masses above 10(8) M-circle dot. We then consider the recently detected common red noise in NANOGrav, PPTA, and EPTA data, working under the hypothesis that it is indeed a stochastic GWB coming from MBHBs. By boosting the massive black hole growth via gas accretion, we show that our model can produce a signal with an amplitude A approximate to (2-3) x 10(-15). There are, however, difficulties in predicting this background level without mismatching key observational constraints such as the quasar bolometric luminosity functions or the local black hole mass function. This highlights how current and forthcoming GW observations can, for the first time, confront galaxy and black hole evolution models.
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